DES16C3cje: A low-luminosity, long-lived supernova

Gutierrez, C. P.; Sullivan, M.; Martinez, L.; Bersten, M. C.; Inserra, C.; Smith, M.; Anderson, J. P.; Pan, Y-C; Pastorello, A.; Galbany, L.; Nugent, P.; Angus, C. R.; Barbarino, C.; Carollo, D.; Chen, T-W; Davis, T. M.; Della Valle, M.; Foley, R. J.; Fraser, M.; Frohmaier, C.; Gonzalez-Gaitan, S.; Gromadzki, M.; Kankare, E.; Kokotanekova, R.; Kollmeier, J.; Lewis, G. F.; Magee, M. R.; Maguire, K.; Moller, A.; Morrell, N.; Nicholl, M.; Pursiainen, M.; Sollerman, J.; Sommer, N. E.; Swann, E.; Tucker, B. E.; Wiseman, P.; Aguena, M.; Allam, S.; Avila, S.; Bertin, E.; Brooks, D.; Buckley-Geer, E.; Burke, D. L.; Rosell, A. Carnero; Kind, M. Carrasco; Carretero, J.; Costanzi, M.; da Costa, L. N.; De Vicente, J.; Desai, S.; Diehl, H. T.; Doel, P.; Eifler, T. F.; Flaugher, B.; Fosalba, P.; Frieman, J.; Garcia-Bellido, J.; Gerdes, D. W.; Gruen, D.; Gruendl, R. A.; Gschwend, J.; Gutierrez, G.; Hinton, S. R.; Hollowood, D. L.; Honscheid, K.; James, D. J.; Kuehn, K.; Kuropatkin, N.; Lahav, O.; Lima, M.; Maia, M. A. G.; March, M.; Menanteau, F.; Miquel, R.; Morganson, E.; Palmese, A.; Paz-Chinchon, F.; Plazas, A. A.; Sako, M.; Sanchez, E.; Scarpine, V.; Schubnell, M.; Serrano, S.; Sevilla-Noarbe, I; Soares-Santos, M.; Suchyta, E.; Swanson, M. E. C.; Tarle, G.; Thomas, D.; Varga, T. N.; Walker, A. R.; Wilkinson, R. (2020): DES16C3cje: A low-luminosity, long-lived supernova. In: Monthly Notices of the Royal Astronomical Society, Vol. 496, No. 1: pp. 95-110

Abstract

We present DES16C3cje, a low-luminosity, long-lived type II supernova (SN II) at redshift 0.0618, detected by the Dark Energy Survey (DES). DES16C3cje is a unique SN. The spectra are characterized by extremely narrow photospheric lines corresponding to very low expansion velocities of less than or similar to 1500 km s(-1), and the light curve shows an initial peak that fades after 50 d before slowly rebrightening over a further 100 d to reach an absolute brightness of M-r similar to 15.5 mag. The decline rate of the late-time light curve is then slower than that expected from the powering by radioactive decay of Co-56, but is comparable to that expected from accretion power. Comparing the bolometric light curve with hydrodynamical models, we find that DES16C3cje can be explained by either (i) a low explosion energy (0.11 foe) and relatively large Ni-56 production of 0.075 M-circle dot from an similar to 15 M-circle dot red supergiant progenitor typical of other SNe II, or (ii) a relatively compact similar to 40 M-circle dot star, explosion energy of 1 foe, and 0.08 M-circle dot of Ni-56. Both scenarios require additional energy input to explain the late-time light curve, which is consistent with fallback accretion at a rate of similar to 0.5 x 10(-)(8) M-circle dot s(-1).

• Item Type: Journal article
• Faculties: Physics
• Subjects: 500 Science > 530 Physics
• ISSN: 0035-8711
• Language: English